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New magnetic field measurements of β Cephei stars and slowly pulsating B stars

Published online by Cambridge University Press:  01 November 2008

Swetlana Hubrig
ESO, Santiago, Chile; email:
M. Briquet
Katholieke Universiteit Leuven, Belgium
P. De Cat
Koninklijke Sterrenwacht van België, Brussel, Belgium
M. Schöller
ESO, Garching, Germany
T. Morel
Université de Liège, Belgium
I. Ilyin
Astrophysikalisches Institut Potsdam, Potsdam, Germany
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We present the results of the continuation of our magnetic survey with FORS 1 at the VLT of a sample of B-type stars consisting of confirmed or candidate β Cephei stars and Slowly Pulsating B stars. Roughly one third of the studied β Cephei stars have detected magnetic fields. The fraction of magnetic Slowly Pulsating B and candidate Slowly Pulsating B stars is found to be higher, up to 50%. We find that the domains of magnetic and non-magnetic pulsating stars in the H-R diagram largely overlap, and no clear picture emerges as to the possible evolution of the magnetic field across the main sequence.

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Copyright © International Astronomical Union 2009


Hubrig, S., Briquet, M., Schöller, M., et al. 2006, MNRAS 369, L61CrossRefGoogle Scholar